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2009/03/13 超新星残骸ワークショップ @ 名古屋大学高等総合研究館 1F カンファレンスホール 大阪大学　常深研究室　 内田 裕之、常深 博、勝田 哲、木村 公、小杉 寛子

白鳥座ループのシェルの観測 + Non-thermal SNR G330.2+1.0 の観測 Shell Structure of the Cygnus Loop + Non-thermal SNR G330.2+1.0. 2009/03/13 超新星残骸ワークショップ @ 名古屋大学高等総合研究館 1F カンファレンスホール 大阪大学　常深研究室　 内田 裕之、常深 博、勝田 哲、木村 公、小杉 寛子 (H. Uchida, H. Tsunemi, S. Katsuda, M. Kimura, H. Kosugi). Outline. Cygnus Loop

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2009/03/13 超新星残骸ワークショップ @ 名古屋大学高等総合研究館 1F カンファレンスホール 大阪大学　常深研究室　 内田 裕之、常深 博、勝田 哲、木村 公、小杉 寛子

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  1. 白鳥座ループのシェルの観測+Non-thermal SNR G330.2+1.0の観測Shell Structure of the Cygnus Loop+ Non-thermal SNR G330.2+1.0 2009/03/13 超新星残骸ワークショップ@名古屋大学高等総合研究館1Fカンファレンスホール 大阪大学　常深研究室　 内田 裕之、常深 博、勝田 哲、木村 公、小杉 寛子 (H. Uchida, H. Tsunemi, S. Katsuda, M. Kimura, H. Kosugi)

  2. Outline • Cygnus Loop • Southwest “Blowout” Region • Abundance Inhomogeneity at the Northern Limb of the Loop • Shell Structure along the Line of Sight • Non-thermal SNR, G330.2+1.0

  3. Cygnus Loop • Location (l,b) = ( 74.0 ,-8.5 ) • Distance 540 pc (Blair et al. 2005) • Age ~10,000 yr • SN Type Core-collapse(Levenson et al. 1997; Tsunemi et al. 2007) • Progenitor Star B0, 15M◎(Levenson et al. 1998) • Cavity Explosion N W ROSAT HRI

  4. Suzaku 32 observations 9 observations ROSAT HRI XMM-Newton Red:0.3-0.5 keV Green: 0.5-1.0 Blue: 1.0-3.0

  5. O VII O VII O VIII O VIII Ne Ne IX IX Ne Ne X X N VI N VI C VI C VI Mg XI Mg XI Si Si XIII XIII Mg XII Mg XII Si Si XIII XIII S XV S XV C C - - band band Fe Fe - - L L Limb North Path North Path South Path South Path Summed Spectra of Cygnus Loop Suzaku XIS0+1+2+3 NXB

  6. Outline • Cygnus Loop • Southwest “Blowout” Region • Abundance Inhomogeneity at the Northern Limb of the Loop • Shell Structure along the Line of Sight • Non-thermal SNR, G330.2+1.0

  7. Cygnus Loop南西領域の観測 South Blowout

  8. Origin of the South “Blowout” Uyaniker et al. (2002)―電波の強度分布から南西に別のSNRの存在を示唆 　→　”blowout”の正体 Aschenbach & Leahy (1999)　－　南西方向のISM密度の薄さが“破れ”の起源

  9. XMM-Newton image POS-8 POS-9 POS-8 OBS_ID 0405490101 date2006/05/13 exp. time 10ks POS-9 OBS_ID 0405490201 date 2006/05/13 Exp. time 10ks Observation of the South Blowout with XMM-Newton × Center of the “extra SNR” (Uyaniker et al. 2002)

  10. 　観測領域を東西に２分割 • 　さらに5,000 photons / regionになるように円環に区切ってスペクトルを調べた true color image POS-8 POS-9 Red: 0.2-0.5 keV Green: 0.5-0.7 keV Blue: 0.7-10 keV

  11. Two component VNEI model High kT component (~0.4keV) Low kT component (~0.2keV) MOS1MOS2 Spatially Resolved Spectral Analysis R=36’ R=95’ • 　各スペクトルは２温度の衝突電離非平衡モデル（VNEI）でよく合う

  12. Tsunemi et al. Uchida et al. East pathWest path Emission Measure Distribution of Fe in the Cygnus Loop Ejecta 2 Tsunemi et al. (2007) EM (1014cm-5) 1 East path Uchida et al. (2008) West path 0 -50 0 50 Distance from the Cygnus Loop Center (arcmin) 高温成分のFeのEMは中心から外へ向けて減少している Feの分布はCygnusLoop中心を通るTsunemi et al.の結果と滑らかに繋がっている →高温成分はCygnusLoopのイジェクタ起源

  13. Two component VNEI model High kT component (~0.4keV) Low kT component (~0.2keV) MOS1MOS2 CygnusLoop南西部のシェルは薄い　 Spatially Resolved Spectral Analysis R=36’ R=95’ • 　各スペクトルは２温度の衝突電離非平衡モデル（VNEI）でよく合う • 　低温成分（~0.2keV）はextra SNRからの放射だとすると温度が低すぎる • 　低温成分はCygnusLoopのシェルからの放射と考えて矛盾はない • 　２温度フィットの結果から、どの領域でもISM成分の寄与は小さい

  14. Origin of the Southwest “Blowout” ~10,000 yrs later... No evidence in X-ray that the nature of the blowout region originated from the extra SNR

  15. Outline • Cygnus Loop • Southwest “Blowout” Region • Abundance Inhomogeneity at the Northern Limb of the Loop • Shell Structure along the Line of Sight • Non-thermal SNR, G330.2+1.0 originated from the large break of the cavity wall

  16. Single Component VNEI model Ne Abundance Katsuda et al. 2008 Uchida et al. 2009 XIS0+XIS1+XIS3 ←SNR center Tsunemi et al. 2009 Suzaku Observations of Limb Regions of the Cygnus Loop C,N,O,Ne等のアバンダンスを調べたところ、一部のリムの外縁部のみがISMの組成に近い

  17. 外縁部に行くほどアバンダンスが高くなっている領域がある外縁部に行くほどアバンダンスが高くなっている領域がある CygnusLoop center

  18. Abundance-enhanced region; typically >0.5solar ~ISM abundance (Katsuda et al. 2008; Tsunemi et al. 2009; Uchida et al. 2009) Abundance-enhanced Region at the Limb of the Cygnus Loop The other limb regions show depleted abundances; typically <0.2solar (Leahy 2004; Miyata et al. 2007; Katsuda et al. 2008; etc.)

  19. The Origin of the Abundance-enhanced Region Interacting with Cloud (Levenson et al. 2002) Interacting with Cloud (Levenson et al. 2005) Lower Ambient Density

  20. The Origin of the Abundance-enhanced Region The blast waves in the abundance-enhanced are now proceeding into the outside of the cavity wall and begin to interact with the surrounding ISM.

  21. Outline • Cygnus Loop • Southwest “Blowout” Region • Abundance Inhomogeneity at the Northern Limb of the Loop • Shell Structure along the Line of Sight • Non-thermal SNR, G330.2+1.0 originated from the large break of the cavity derived from the breakout or the thinness of the cavity

  22. RegionB RegionA 低温成分の寄与の違い 視線方向のシェルの厚みを反映 low kT component - cavity material origin high kT component - ejecta origin

  23. Thin Shell Region flux of low-kT component flux of high-kT component total flux Previous Study (Kimura et al. 2009) Flux Distribution Flux (counts cm-2s-1arcmin-2) Distance from center (arcmin) “Blowout” may exist here along the line of sight

  24. Suzaku: 29 observations XMM: 9observations ~10,000 counts / region 949 box regions are obtained Each spectrum is fitted by single component VNEI or two component VNEI Flux of each component is calculated 2D Flux Distribution Map

  25. Rim-brightning V shape structure (Leahy 2004) 0.2-3.0 keV Flux Distributions of Low- and High-kT Component in unit of counts cm-2s-1arcmin-2 Low-kT component High-kT component

  26. Low-flux region with radius ~30 arcmin Blowout region has the lowest flux 0.2-3.0 keV Flux Distributions of Low- and High-kT Component “Blowout” also exists in the middle west along the line of sight in unit of counts cm-2s-1arcmin-2 Low-kT component High-kT component

  27. Outline • Cygnus Loop • Southwest “Blowout” Region • Abundance Inhomogeneity at the Northern Limb of the Loop • Shell Structure along the Line of Sight • Non-thermal SNR, G330.2+1.0 originated from the large break of the cavity derived from the breakout or the thinness of the cavity showed that the “blowout” also exists in the direction of our line of sight in the middle west of the Loop

  28. Color Image: Chandra ACIS(0.5-10.0keV) Contour: MOST(843MHz) Non-thermal SNR G330.2+1.0 Southwestern Limb Easter Limb Thermal model ~0.7keV Powerlaw Γ~2.3 Powerlaw Γ~2.5 Radio Intensity: High X-ray Intensity: Low Radio Intensity: Low X-ray Intensity: High Non-thermal emission was first detected with ASCA (Torii et al. 2006) Thermal emission are detected at the eastern limb (Park et al. 2008) Anti-correlation between the X-ray and radio intensities

  29. Summary • Cygnus Loop • Southwest “Blowout” Region • Abundance Inhomogeneity at the Northern Limb of the Loop • Shell Structure along the Line of Sight • Non-thermal SNR, G330.2+1.0 originated from the large break of the cavity derived from the breakout or the thinness of the cavity showed that the “blowout” also exists in the direction of our line of sight in the middle west of the Loop

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